In this paper, we are going to study the above mentioned massive scalar perturbation in the context of rotating braneworld black holes. Braneworld black holes are natural candidates to study quantum black holes [1]}, [2]}, [3]}, [4]}. Recently these solutions are extensively used in ECO phenomenology [2]}, tidal heating of black holes [6]}, optical properties of black holes [7]} and in some other interesting cases [8]}, [9]}, [10]}, [11]} . These black hole solutions differ from their counterpart in general relativity by the presence of a tidal charge, unlike electric charge tidal charge can take negative values, which has no analogue in GR. This charge depends on the electric part of the bulk Weyl tensor and carries the effect of extra dimensions. An immediate consequence of tidal charge is that in the case of extremal Kerr-like black holes we do not have a=M, where a is the black hole spin parameter and M is the mass parameter. Moreover, \(a>M\)  is allowed, which is also absent in GR. As mentioned before, some earlier works [12]}, [13]}, [14]} have shown that the superradiant instability growth rate of massive scalar perturbation of rotating black holes is maximum for extremal black holes. Here we will do a superradiant stability analysis for rotating braneworld black holes under massive scalar perturbation. That is, we will try to determine a parameter space where braneworld Kerr-like (or Kerr-Newman like) black holes are superradiantly stable under massive scalar (or charged massive scalar) perturbations. To do the analysis we will follow the formalism presented in [15]}, [16]}, [17]}. As stated before, superradiant instability happens when there exists a local minima (that is trapping well) of effective potential outside the horizon. So for stability under superradiance there should exist only one maxima of effective potential outside the horizon. This is the key argument of our analysis. In this analytic treatment, we will consider only the real frequencies of the scalar wave. But the conclusions can be extended to nearly real frequencies as in [18]}, [19]}, [12]}. Like [18]} we will assume that both the superradiance condition and the bound state condition hold simultaneously. In the case of Kerr-like extremal braneworld black holes, we will obtain a bound on tidal charge for superradiant stability under a massive scalar perturbation. Similarly, for Kerr-Newman like extremal braneworld black holes, we will obtain a lower bound of the product of mass to charge ratio of the black hole and scalar field for which the system is superradiantly stable.
